[29.08] Hydrodynamics of Radioactivity Injection into the Presolar Cloud

K. W. Davis, M. D. Leising (Clemson University)

Live short-lived radionuclides detected in early solar
system materials constrain the time between their creation
and the formation of solids in the early solar system. The
travel time from a stellar source and time for the presolar
cloud to start condensing into solids would seem to take too
long for radionuclides with lifetimes of only a few Myr to
still be alive. Among several possible explanations is a
supernova explosion near the presolar cloud both seeding the
cloud with the short-lived radionuclides and initiating
cloud collapse. Several of the detected short-lived
radionuclides are only found deep within the supernova
material, begging the question of how they become
incorporated into a molecular cloud when the ISM and outer
layers of ejecta lie between them and the cloud. Some have
proposed that hydrodynamic instabilities can inject the
appropriate material into the cloud. We perform simulations
using the Zeus-2D hydrodynamic code to investigate the
effect of hydrodynamic instabilites on injection of
supernova material into a cold molecular cloud. We model the
supernova as a hot, high density bubble of gas allowed to
expand into the ISM and collide with a cold dense cloud and
give it a very low value of angular momentum to distiguish
its material from the ambiant ISM and cloud material.

The author(s) of this abstract have provided an email address
for comments about the abstract:
kwdavis@clemson.edu